“elementary particles” lecture 2

Niels Tuning (1)

“Elementary Particles” Lecture 2

Niels Tuning

Harry van der Graaf

Ernst-Jan Buis

Martin Fransen

Niels Tuning (2)

Fundamental

Physics

Astrophysics Cosmics Grav Waves Neutrinos

Quantum Mechanics

Special

Relativity

General

Relativity

Forces

Particles

Gravity

Interactions with Matter

Bethe Bloch Photo effect Compton, pair p. Bremstrahlung Cherenkov

Light Scintillators PM Tipsy Medical Imag.

Charged Particles

Si Gaseous Pixel

Optics

Experiments ATLAS Km3Net Virgo Lisa …

Detection and sensor techn. Theory

Quantum

Field Theory

Accelerators Cyclotron X-ray Proton therapy

Niels Tuning (3)

Fundamental

Physics

6) Ernst-Jan Astrophysics

2) Niels Quantum Mechanics

1) Niels Special Relativity

9) Ernst-Jan General Relativity

Niels 7) + 10) Forces 5) + 8) Particles

9) Ernst-Jan Gravity

3) Harry RelativisticInteractions with Matter

4) Harry Light

11) +12) Martin Charged Particles

9) Ernst-Jan Optics

6) + 9) Ernst-Jan Martin 13) + 14) Excursions Experiments

Detection and sensor techn. Theory

2) Niels Quantum Field Theory

1) Harry Accelerators

1)  11 Feb: Accelerators (Harry vd Graaf) + Special relativity (Niels Tuning)

2)  18 Feb: Quantum Mechanics (Niels Tuning)

3)  25 Feb: Interactions with Matter (Harry vd Graaf)

4)  3 Mar: Light detection (Harry vd Graaf)

5)  10 Mar: Particles and cosmics (Niels Tuning)

6)  17 Mar: Astrophysics and Dark Matter (Ernst-Jan Buis)

7)  24 Mar: Forces (Niels Tuning)

8)  21 Apr: e+e- and ep scattering (Niels Tuning)

9)  28 Apr: Gravitational Waves (Ernst-Jan Buis)

10) 12 May: Higgs and big picture (Niels Tuning)

11) 19 May: Charged particle detection (Martin Franse)

12) 26 May: Applications: experiments and medical (Martin Franse)

13) 2 Jun: Nikhef excursie

14) 8 Jun: CERN excursie

Schedule

Niels Tuning (4)

Thanks

•  Ik ben schatplichtig aan: –  Dr. Ivo van Vulpen (UvA)

–  Prof. dr. ir. Bob van Eijk (UT)

–  Prof. dr. M. Merk (VU)

Niels Tuning (5)

1)  Intro: Standard Model & Relativity

2)  Basis 1)  Atom model, strong and weak force

2)  Scattering theory

3)  Hadrons 1)  Isospin, strangeness

2)  Quark model, GIM

4)  Standard Model 1)  QED

2)  Parity, neutrinos, weak inteaction

3)  QCD

5)  e+e- and DIS

6)  Higgs and CKM

Niels Tuning (6)

1900-1940

1945-1965

1965-1975

1975-2000

2000-2015

18 Feb

10 Mar

24 Mar

21 Apr

12 May

11 Feb

Exercises Lecture 1: Special Relativity

Niels Tuning (7)

x’ = ct’

Niels Tuning (8)

Niels Tuning (9)

Niels Tuning (10)

2 Relativistic momentum

a) Using E = mc2 and p = mv, one finds:E2/c2 − p2 = m2c2 − m2v2 = m2(c2 − v2) = m2c2

b) Using E = γm0c2 and p = γm0v, one finds:

E2/c2 − p2 = γ2(m2(c2 − v2)) = m2c2 1−v2/c2

1−v2/c2 = m2c2.

2 Relativistic momentum

Given 4-vector calculus, we know that pµpµ = E2/c2 − p2 = m20c

a) Show that you get in trouble when you use E = mc2 and p = mv.

b) Show that E = γm0c2 and p = γm0v obey E2/c2 − p2 = m20c2.

Notice that energy and momentum are “treated” in the same way; both get an extrafactor γ. Such an “identical treatment” is known as covariance, and implies that theLorentz transformations and 4-vector description yield a consistent picture.

It is tempting to write the substitution m = γm0, to yield the original formulas E = mc2

and p = mv. This is sometimes referred to as “relativistic mass”. However, AlbertEinstein himself wrote on 19 June 1948 in a letter to Lincoln Barnet (quote from L.B.Okun (1989), p. 42): “It is not good to introduce the concept of the mass m = γm0 of amoving body for which no clear definition can be given. It is better to introduce no othermass concept than the rest mass m0. Instead of introducing m it is better to mention theexpression for the momentum and energy of a body in motion.”

So, from now on every m we use, refers to the rest mass m0. And we will use naturalunits, c = 1. Hence, E = γm !

Niels Tuning (11)

3 Center-of-mass energy

a) Not only the space and time can be expressed as a 4-vector, but also energy andmomentum can be expressed as 4-vectors, pµ = (E/c, px, py, pz). Because pµpµ isinvariant, this means that the rest-mass m0 of a particle does not change underLorentz transformations. Show that pµpµ = m2

b) Let’s consider two colliding particles a and b, with 4-momenta pµa and pµ

b . We willuse natural units, with c = 1 and ! = 1, so pµ

a = (Ea, pa). We take the masses ofthe two colliding particles equal, ma = mb = m, and we sit in the center-of-massframe of the system, pa = −pb. What are the four components of the sum of thetwo 4-vectors, pµ

tot = (pµa + pµ

c) The ’invariant mass’ of the combined system, is often called the ’center-of-massenergy’ of the collision. If the energy of both particles a and b is 4 TeV, what isthen the center-of-mass energy,

√s ≡

pµtotpµ,tot ?

d) Let’s consider a fixed-target collision of two protons. One proton has an energy of4 TeV, and 4-vector pµ

a , whereas the other proton is at rest, with 4-vector pµb . What

are the four components of the sum of the two 4-vectors, pµtot = (pµ

a + pµb ) ? Give

the expression for the center-of-mass energy of this system.

e) People were afraid that the earth would be destroyed at the start of the LHC,planning for collisions with beams of 7 TeV each. The earth has been bombardedfor billions of years with cosmic rays. What is the center-of-mass energy of thehighest energetic cosmic rays ( 1021 eV) hitting the atmosphere? Was the fearjustified?

f) What is the energy of a cosmic ray hitting the atmosphere, that corresponds to thecenter-of-mass energy of collisions of two lead-ions 208Pb with energies of 2.24 TeVper nucleon?

g) Consider relatively low-energy proton-proton collisions, with opposite and equalmomenta (ie. the center-of-mass system is at rest). In the process p+p → p+p+p+pan extra proton-antiproton pair is created. What is the minimum energy of theprotons to create two extra (anti)protons?

Niels Tuning (12)

•  Standard Model Lagrangian

•  Standard Model Particles

Lecture 1: Standard Model & Relativity

Niels Tuning (13)

•  Theory of relativity –  Lorentz transformations (“boost”)

–  Calculate energy in colissions

•  4-vector calculus

•  High energies needed to make (new) particles

Lecture 1: Standard Model & Relativity

Niels Tuning (14)

•  Quantum mechanics: equations of motions of wave functions –  Schrodinger, Klein Gordon, Dirac

•  Forces –  Strong force, pion exchange

–  Weak nuclear force, decay

•  Scattering Theory –  Rutherford (classic) and QM

–  “Cross section”

–  Coulomb potential

–  Yukawa potential

–  Resonances

Outline for today

Niels Tuning (15)

•  Lecture 1: –  ch.3 Relativistic kinematics

•  Lecture 2: –  ch.5.1 Schrodinger equation –  ch.7.1 Dirac equation

–  ch.6.5 Scattering

•  Lecture 3: –  ch.1.7 Quarkmodel

–  ch.4 Symmetry/spin

•  Lecture 4: –  ch.7.4 QED

–  ch 11.3 Gauge theories

•  Lecture 5: –  ch.8.2 e+e-

–  ch.8.5 e+p

•  Lecture 6: –  ch.11.8 Higgs mechanism

D. Griffiths “Introduction to Elementary Particles”

Niels Tuning (16)

•  Introduce “matter particles” –  spinor ψ from Dirac equation

•  Introduce “force particles”

•  Introduce basic concepts of scattering processes

Lecture 2: QM, Dirac and Scattering

Niels Tuning (17)

Quantummechanics

From classic to quantum

•  The wavefunction ψ describes a system (eg. particle)

•  Physical quantities are given by operators

Niels Tuning (19)

Why does the black body spectrum look like it does?

Why does the electron not fall onto the nucleus?

! Finite number of wavelengths ( E=hν ) ! Finite number of nuclear orbits

•  In QM a particle is not localized

•  Probability of finding a particle somewhere in a volume V of space:

•  Probability to find particle anywhere in space = 1

Ø  condition of normalization:

Wavefunction

Niels Tuning (20)

dVtdVtP 2),(),( rr Ψ=

2=Ψ∫

spaceall

Each particle may be described by a wave function ψ(x,y,z,t), real or complex, having a single value for a given position (x,y,z) and time t

Any physical quantity is associated with an operator §  An operator O: the “recipe” to transform ψ into ψ’

–  We write: Oψ = ψ’

•  If Oψ = oψ then –  ψ is an eigenfunction of O and

–  o is the eigenvalue.

We have “solved” the wave equation Oψ = oψ by finding simultaneously ψ and o that satisfy the equation. Ø  o is the measure of O for the particle in the state described by ψ

Operator

Niels Tuning (21)

•  What operator belongs to which physical quantity?

Correspondence?

Niels Tuning (22)

Classical quantity QM operator

Let’s try operating:

• Wavefunction:

• Momentum operator :

• Or energy operator:

Example

Niels Tuning (23)

( ) tikxAetkxitkxAtx ωωω −=−+−=Ψ ]sin[]cos[),(

),(),(ˆ )()()( txkkAeikAei

txp tkxitkxitkxix Ψ===

∂=Ψ −−−

!!!! ωωω

( ) ( )txEAeAeiiAet

itxE tkxitkxitkxi ,)(,ˆ )()()( Ψ==−=∂

∂=Ψ −−− ωωω ωω !!!

Ø  Ψ is indeed eigenfunction (ђk and ђω are the eigenvalues for ˆp and ˆE)

Average value of physical quantity: expectation value

Example:

Expectation value

Niels Tuning (24)

[ ]∫+∞

∞−

ΨΨ= dxtxWtxW ),(ˆ),(*

[ ] [ ]

[ ] [ ] [ ] [ ] pkdxAeAekdxAeiki

dxAexi

dxAeAedxxAex

ikxikxikxikx

ikxikx

ikxikxikx

⎥⎦

⎤⎢⎣

⎡∂

∞→→

∫∫

∞−

n integratio of limits as 0 where

,1)( with )( ψψ

Think of the Staatsloterij:

EUR41.950.13697.0)()(prize win that y toprobabilit:)(

prize:

=×==∑i

xpxXExp

Heisenberg How to describe a particle that is “localized” somewhere, but which is also “wave-like” ?

Ø k can be any value:

Ø Fourier decomposition of many frequencies Ø  The more frequencies you add, the more it gets localized

Ø  The worse you know p, the better you know x !

Niels Tuning (25)

ikxAe=ψ

Heisenberg

Niels Tuning (26)

How to describe a particle that is “localized” somewhere, but which is also “wave-like” ?

Ø Fourier decomposition of many frequencies Ø  The more frequencies you add, the more it gets localized

Ø  The worse you know p, the better you know x !

Twitter

Niels Tuning (27)

•  Uncertainty relation à Commutation relation Ø  A wave function cannot be simultaneously an eigenstate of position

and momentum

•  Suppose it was, what then?? Ø  Then the operators would commute:

Heisenberg

Niels Tuning (28)

( ) ( ) ( ) 0000000 =Ψ−=Ψ−=Ψ− pxpxXpxPXPXP xxx

Schrödinger

Niels Tuning (29)

Classic relation between E and p:

Quantum mechanical substitution:

(operator acting on wave function ψ)

Schrodinger equation:

Solution:

(show it is a solution)

•  Polar coordinates

•  Separate variables

•  Three differential equations for R, φ, θ:

•  Radial Schrödinger equation –  Potential is augmented by “centrifugal barrier” :

Intermezzo: “radial Schrödinger equation”

Niels Tuning (30)

Linear momentum Potential energy Angular momentum

(apparent centrifugal force)

Klein-Gordon

Niels Tuning (31)

Relativistic relation between E and p:

Quantum mechanical substitution:

(operator acting on wave function ψ)

Klein-Gordon equation:

Solution:

But! Negative energy solution?

with eigenvalues:

Paul Dirac tried to find an equation that was §  relativistically correct,

§  but linear in d/dt to avoid negative energies

§  (and linear in d/dx (or ∇) for Lorentz covariance)

He found an equation that §  turned out to describe spin-1/2 particles and

§  predicted the existence of anti-particles

Niels Tuning (32)

Niels Tuning (33)

Write Hamiltonian in general form,

but when squared, it must satisfy:

Let’s find αi and β !

So, αi and β must satisfy:

§  α12 = α2

2 = α32 = β2

§  α1,α2,α3, β anti-commute with each other

§  (not a unique choice!)

Ø  How to find that relativistic, linear equation ??

Niels Tuning (34)

So, αi and β must satisfy:

§  α12 = α2

2 = α32 = β2

§  α1,α2,α3, β anti-commute with each other

§  (not a unique choice!)

The lowest dimensional matrix that has the desired behaviour is 4x4 !?

Often used

Pauli-Dirac representation:

Ø  What are α and β ??

Usual substitution:

Leads to:

Multiply by β:

Gives the famous Dirac equation:

Niels Tuning (35)

(β2=1)

The famous Dirac equation:

R.I.P. :

Niels Tuning (36)

Remember!

§  µ : Lorentz index

§  4x4 γ matrix: Dirac index

Less compact notation:

Even less compact… :

Niels Tuning (37)

Ø  What are the solutions for ψ ??

•  Transformation of contravariant 4-vector:

•  Lowering the index, costs minus-sign:

•  Transformation of covariant 4-vec:

Ø  Derivative ∂µ= ∂/∂xµ transforms as covariant 4-vec (consistent with index):

Ø  And:

Intermezzo: The “Four-derivative”

Niels Tuning (38)

(Sum over index υ)

(E,-p)→iћ(∂/∂t,∇)

Griffiths, p.214:

Niels Tuning (39)

Solutions to the Dirac equation?

Try plane wave:

Linear set of eq:

Ø  2 coupled equations:

If p=0:

Niels Tuning (40)

Try plane wave:

If p≠0:

Two solutions for E>0:

(and two for E<0)

Tuning (41)

Try plane wave:

If p≠0:

Two solutions for E>0:

(and two for E<0)

( )⎟⎟⎟⎟⎟

⎜⎜⎜⎜⎜

mEpu !!

( )⎟⎟⎟⎟⎟

⎜⎜⎜⎜⎜

Niels Tuning (42)

ψ is 4-component spinor

4 solutions correspond to fermions and anti-fermions with spin+1/2 and -1/2

Needed e.g. to calculate the probability for a scattering process like:

Ø  What do we need this for ??

•  Dirac found his equation in 1928

•  The existence of anti-matter was not taken serious until 1932, when Anderson discovered the anti-electron: the positron

Prediction of anti-matter

Niels Tuning (43)

Discovery of anti-matter

Niels Tuning (44)

Lead plate

positron

Nobelprize 1936

•  Discovery of the neutron, by J. Chadwick

Ø  What was known at that time about the nucleus?

What else happened in 1932 ?

Niels Tuning (45)

Nobelprize 1935

Rutherford

Thomson

Measurement:

Hypothesis:

dσdΩ(θ) =

ZZ '4E⎛

⎝ ⎜

⎠ ⎟ 2 1sin4 θ /2( )

V ∝1r

‘Bullet’: 6 MeV alpha particle

It was as if you fired a 15-inch shell at a sheet of tissue paper and it came back to hit you.

Number of back-scattered particles ~ A3/2

‘Hey, that is funny… looking at Rutherford’s results, one notices that the number of electrons per atom is precisely halve the atom mass.’ (Note: Proton only proposed in 1920) Antonius van den Broek

July 1911

•  Discovery of the neutron, by J. Chadwick

1)  Neutral §  Gamma? No! protons too energetic

2)  mn ~ mp

Ø  Interpretation:

What else happened in 1932 :

Niels Tuning (48) Nobelprize 1935

radiation ionizing-non→+ Beα

CnBeHe 126

42 +→+

(lots of H)

Towardsmassiveforcecarriers

•  1932: discovery of neutron

§  α+ 9Be → n + 12C

§  Nuclear effect only à short range

Ø What can you then deduce about: §  Energy scale

§  Potential

Strong interaction

Niels Tuning (50)

•  1935: Introduced strong carriers on small distances

•  Massive particle, that exists only shortly –  ‘virtual’ particle

Yukawa

Niels Tuning (51)

Compare:

•  Electro-magnetism

•  Infinite range

•  Transmitted by massless photon

Ø  Coulomb potential

•  Strong force

•  Finite range

•  Transmitted by massive pion

Ø  Yukawa potential

R: range

R→ ∞

•  1935: Introduced strong carriers on small distances

•  Massive particle, that exists only shortly –  ‘virtual’ particle

Yukawa

Niels Tuning (52)

•  Strong force

•  Finite range

•  Transmitted by massive pion

Ø  Yukawa potential

R: range

Yukawa’sstrongnuclearforce

Shortrange:massivequanta

Whatisthetypicalmassthatlimitstherangetotheprotonradius(10-15m)?

Couplingg2>α

Strength:couplingconstant

r1V :Coulomb α−∝

α =e2

4πε0hc=

1137.04

Rr /2V :Yukawa

−∝

= 200 MeV €

Δt = Δr /c → Δt ~ 3⋅ 10−24 s

ΔE =hΔt

= 3⋅ 10−11J

Heisenberg :ΔEΔt > h

Homework

Yukawa’s pions – pictures Powell used a new detection technique Photographic emulsion: - Thick photosensitive film - Charged particles leave tracks Results: two particles (pion and muon)

Ø 1947Discoveryofpion(Powell):Nobelprijs1950Ø 1935Predictionofpion(Yukawa): Nobelprijs1949

§  π-meson, m=140 MeV, short lifetime Produced high in atmosphere and decays before reaching sealevel.

§  muon (µ), m=105 MeV, long lifetime Reaches sea-level and weakly interacts with matter

π+ →µ+υµ

µυυµ ++→ ++ee

Intermezzo: Strong force nowadays:

Niels Tuning (55)

Ø  Yukawa:

“Effective” description

Still useful to describe some features!

In particular at “lower energies”

Ø  Gluons:

More fundamental description

But fails at low energies…

Intermezzo: Strong force nowadays:

Niels Tuning (56)

Ø  Yukawa:

“Effective” description (≠ wrong!)

Still useful to describe some features!

In particular at “lower energies”

Ø  Gluons:

More fundamental description

But fails at low energies…

•  1895: Röntgen discovered radiation from vaccum tubes (γ)

•  1895: Bequerel measured radiation from 238U (n)

•  1898: Curie measured radiation from 232Th (α)

•  1899: Rutherford concluded α ≠ β •  1914: Rutherford determined wavelength of γ (scattering of crystals)

Radioactive decay

Niels Tuning (57)

•  β-decay: weak interaction –  W-exchange

•  α-decay: strong interaction –  Pions (gluons?!) keeps nucleus together

•  γ-decay: electro-magnetic interaction –  Excited states

Link with Modern physics

Niels Tuning (58)

1)Numberofdecayedparticles,dN,isproportionalto:N,dtandconstantΓ:tt+dt

2)  Statesthatdecay,donotcorrespondtoonespecificenergylevel,buthavea“width”ΔE:

lifetime

Heisenberg:

Ø Thewidthofaparticleisinverseproportionaltoitslifetime!

ParticleDecay

Quantummechanicaldescriptionofdecay

StatewithenergyE0()andlifetimeτToallowfordecay,weneedtochangethetime-dependence:

What is the wavefunction in terms of energy (instead of time) ? Ø  Infinite sum of flat waves, each with own energy Ø Fourier transformation:

( ) ⎟⎠

⎞⎜⎝

⎛ Γ−−Ψ=

0 iEEi

ProbabilitytofindparticlewithenergyE: Breit-Wigner

E0-Γ/2 E0E0-Γ/2

Pmax/2

Resonance-structurecontainsinformationon:§ Mass§ Lifetime§ Decaypossibilities

Resonance

Scattering

•  Quantum mechanics: equations of motions of wave functions –  Schrodinger, Klein Gordon, Dirac

•  Forces –  Strong force, pion exchange

–  Weak nuclear force, decay

•  Scattering Theory –  Rutherford (classic) and QM

–  “Cross section”

–  Coulomb potential

–  Yukawa potential

–  Resonance

Outline for today

Niels Tuning (63)

•  Decay

–  Decay width is reciprocal of decay time:

–  Total width is sum of partial widths:

–  Branching fraction for certain decay mode:

–  Unit: inverse seconds

•  Scattering

–  Parameter of interest is “size of target”, cross section σ

–  Total cross section is sum of possible processes:

–  Unit: surface

Ø  Golden rule:

Decay and Scattering: decay width and cross section

Niels Tuning (64)

τ = 1/Γ

Γtot = ΣiΓi

BR = Γi / Γtot

σtot = Σiσi

a → b + c

a + b → c + d

Fermi's“goldenrule”gives:Thetransitionprobabilitytogofrominitialstateitofinalstatef

Fermi’sGoldenRule

density of final states

Amplitude M: contains dynamical information fundamental physics

Phase space φ contains kinematic information masses, momenta

Rutherford

Niels Tuning (66)

•  Classical calculation of cross section

of a scattering process

•  Scatter from spherical potential

•  Incoming: impact parameter between b and db

•  Outgoing: scattering angle between θ and dθ

Ø  3d: incoming particle “sees” surface dσ, and scatters off solid angle dΩ

Rutherford

Niels Tuning (67)

Ø  Calculate:

Rutherford

Niels Tuning (68)

§  Conservation of angular momentum:

§  Force:

Rutherford

Niels Tuning (69)

Before After:

(v=rω)

§  Conservation of angular momentum:

§  Force:

Rutherford

Niels Tuning (70)

Before After:

=(cosθ + 1)

Replace r by b,

using L conservation

•  Differential cross section

Rutherford scattering à Cross section

Niels Tuning (71)

•  Luminosity L Ø  L = dN/dσ Ø  Number of incoming particles per unit surface

•  Describe a stationary state, that satisfies the incoming and outgoing wave

Scattering Theory: QM

Niels Tuning (72)

V≠0 k2=2mE

•  Find a solution which is a superposition of the incoming wave, and the outgoing waves

Scattering Theory: QM

Niels Tuning (73)

Incoming plane wave

Outgoing spherical wave

ingoing outgoing

•  Superposition of incoming wave and outgoing waves

•  Scattering amplitude f calculated from potential V

–  Fourier transform of potential:

Scattering Theory: Quantum mechanics

Niels Tuning (74)

Classical: QM:

Incoming plane wave

ingoing outgoing

•  Yukawa:

•  Coulomb:

•  Centrifugal Barier:

Scattering Theory: Quantum mechanics

Niels Tuning (75)

Classical: QM:

Incoming plane wave

Well-known resonances

Z-boson

e+e-cross-section

e+e-→R→ e+e-

π+p→R→ π+p

More resonances

•  That is how we see and discover particles!

•  As resonances!

Why did we need this mathematical trickery?

Niels Tuning (78)

•  How to calculate amplitude M ?

•  The ‘drawing’ is a mathematical object!

Feynman Rules

Niels Tuning (79)

M= g g

1/(q2-m2)

Twitter

Niels Tuning (80)

1)  Intro: Standard Model & Relativity

2)  Basis 1)  Atom model, strong and weak force

2)  Scattering theory

3)  Hadrons 1)  Isospin, strangeness

2)  Quark model, GIM

4)  Standard Model 1)  QED

2)  Parity, neutrinos, weak inteaction

3)  QCD

5)  e+e- and DIS

6)  Higgs and CKM

Niels Tuning (81)

1900-1940

1945-1965

1965-1975

1975-2000

2000-2015

18 Feb

10 Mar

24 Mar

21 Apr

12 May

11 Feb

Extra: derivation of scattering amplitude f

Niels Tuning (82)

Scattering Theory

Niels Tuning (83)

•  Incoming particle (almost) free:

•  Introduce Green function such:

•  If we know G, then the solution for

•  is indeed a sum of the 2 waves:

•  With:

Scattering Theory

Niels Tuning (84)

•  Large r:

•  f: “scattering amplitude”:

•  which we will use for:

Ø  Differential equation became integral equation, but how do we solve it??

Scattering Theory

Niels Tuning (85)

•  f: “scattering amplitude”:

•  which we will use for:

•  1st approximation:

Ø  How do we solve it?? Not analytic… è Perturbation series!

Ø  Scattered wave is described by Fourier transform of the potential

•  Let’s try the Yukawa potential

Scattering Theory

Niels Tuning (86)

•  Yukawa:

•  Coulomb (aà0) :

Ø  We found back the classical solution from Rutherford

Interpretation

Niels Tuning (87)

ingoing outgoing

•  Consider again the amplitude: (Fourier transform of potential)

•  We used quantum mechanics,

•  but with relativistic quantum field theory, the concept is similar:

Feynman diagram

•  Let’s try an effective potential:

Scattering Theory

Niels Tuning (88)

Ø  We found the non-relativistic Breit-Wigner resonance formula!

Scattering to this potential can lead to a bound system, that can then “tunnel away”

Discoverypions/muons

Discoveryanti-matter

Discovery‘strange;particles

Usecosmicrays

“elementary particles” lecture 2

Documents

elementary particles in super string theory

chapter 43 elementary particles. high-energy particles and...

elementary particles: building blocks of...

general physics (phy 2140) lecture 20 modern physics...

classification of the elementary particles. hyperons

elementary particles in physics

elementary particles in curved spacetime

composite model of elementary particles

fields and elementary particles

atoms, nuclei, elementary particles, and...

elementary particles and bubble chambers · elementary...

historical introduction to elementary particles: leptons and...

lecture 21 - wayne state...

general physics (phy 2140) lecture 21 modern physics...

lecture 4.4 – particles to particles and complex...

elementary particles in physics - physics &...

elementary particles and high energy physics

the mysterious standard model of elementary particles

how elementary are the elementary particles? the science

discovering elementary particles and determining...